地震间隙图像与地震大趋势   总被引：2，自引：2，他引：0       下载免费PDF全文

王周元  何少林  彭伟荣  姬凤英 《地震工程学报》1998,20(4):57-62

分析了几个区域的地震间隙图像特征及其与地震大形势的关系。本世纪６０年代前全球 历了大震活跃期,地震间隙基本保持平稳均匀分布,之后活动减弱、转平静。  相似文献   

红河断裂北段土壤中断层气含量变化特征   总被引：1，自引：0，他引：1       下载免费PDF全文

颜鹍  李如陶  李四海  尤伟 《地震工程学报》1998,20(3):89-91

介绍了作者在滇西地震预报实验场区进行的土壤中断层气研究结果．沿红河断裂带断层气组分Ｈ２,ＣＯ２,Ｈｇ和Ｒｎ含量很高．沿该断裂洱源测线断层气Ｈ２,ＣＯ２和Ｒｎ含量最低,向南Ｈ２,ＣＯ２含量逐渐升高,其中以定西岭测线的Ｈ２,ＣＯ２含量最高．表明在该段断裂活动强烈,而洱源一带断裂活动较弱．  相似文献   

利用地震活动性分析对张北-尚义地震进行预测与震后反思   总被引：1，自引：0，他引：1       下载免费PDF全文

董瑞树  任国强 《地震地质》1998,20(2):27-130

从地震活动性分析对张北－尚义地震所作的中长期预测进行总结与反思。首先通过张北－尚义地震所在的燕山－渤海北西向地震带的地震活动性分析,对该带作了分段,并确认了张家口段为未来中强震的危险段。第二步通过ＴＢＢ法计算确认了该段内２８号潜源为１～３ａ的危险区,该区靠近张北震中区,此次地震震中即在使用资料范围内。第三步,由对预报结果的反思,提出应加强中强地震构造背景的研究,特别要注意区域地震活动  相似文献   

震群活动和地震预报综述   总被引：1，自引：0，他引：1  

宋俊高  王炜 《国际地震动态》1998,(9):6-11

研究震群和大地震的关系、用前兆震群预报未来地震的发生,是世界范围内比较活跃的课题之一。文章例举了震群的一些指标以说明前兆性震群的预报意义,并从大范围的众多震群活动阐述大震前震群活动的一些特征。根据震群的分布可确定未来大震的发生地点,并解释不同类型震群的力学成因。  相似文献   

山东中部一条明显的北西向中强地震带   总被引：1，自引：0，他引：1  

晃洪太  李家灵 《华北地震科学》1998,16(2):23-29

长清－临沂地震带是山东中部一条明显的北西向中强地震带,由９次中强地震组成。这些地震沿北西向展布,主要分布在四个震源区,大致呈５０￣５５ｋｍ等间距分布。除１６６８年郯城地震与北北东向的郯庐断裂带有关外,其它地震受北西向蒙山断裂控制,是该断裂各为层段新活动的结果。另外,该地城带内地震的发生还有一定深部构造背景。未来应注意研究该带内再次发生中强地震的可能。  相似文献   

太白维山火山岩系序列相划分及火山活动特征   总被引：4，自引：0，他引：4  

王建新  李景春 《华北地质矿产杂志》1998,13(2):118-125

太白维山火山岩系为晋东北地区中生代火山断陷盆地产物。通过工作研究,确定陈我内岩系的岩石类型及空间分布;指出了两大岩系为两个岩浆源的产物及各序列相的成因类型;确定了水下火山碎屑涌流相的存在,并提出了对形成岩浆蒸气爆发岩的新认识。  相似文献   

辽西地区中生代义县旋回火山活动特征分析   总被引：6，自引：0，他引：6  

史卜庆  吴智平 《高校地质学报》1998,4(4):413-422

辽西地区广泛发育中生代火山岩,其中以义县旋回火山岩最为发育。本文在对辽西地区义县旋回火山岩微量元素地球化学特征研究的基础上,认为义县旋回火山岩具有同源性质,由壳幔混溶物质作用于统一的火山活动过程中产生。  相似文献   

宝石颜色的命名与判定方法评述     

张庆麟 《上海国土资源》1998,(3):24-29

较系统评述了现有的各种命名与判定宝石颜色的方法,如命名法中的二名法、类似法、色度法和三要素法;判定法中的目测法、仪器测量法和对比法。指出它们均存在有不同程度的缺点,但相对比较起来,用色谱图系的对比法是目前较好的方法。  相似文献   

A new population of brown dwarfs     

M. R. S. Hawkins  C. Ducourant  H. R. A. Jones  & M. Rapaport 《Monthly notices of the Royal Astronomical Society》1998,294(3):505-512

In this paper we report the first results from a survey for low-mass stars and brown dwarfs, based on a photographic stack of around 100 Schmidt plates. This survey extends photographic searches by about 2 mag, and covers an area of 25 deg². Some 30 faint objects with large R − I colours were selected for further study, and were found to have very strong molecular absorption in their spectra, but only moderately red infrared colours. Five of these stars were selected for a parallax programme; three of these were found to be at a distance of around 45 pc, implying a very low luminosity. On the basis of their luminosity alone it is clear that these stars are field brown dwarfs, and we discuss their likely evolutionary status in the context of current models of low-mass stellar evolution.  相似文献   

The light curves of soft X-ray transients     

King  & Ritter 《Monthly notices of the Royal Astronomical Society》1998,293(1):L42-L48

We show that the light curves of soft X-ray transients (SXTs) follow naturally from the disc instability picture, adapted to take account of irradiation by the central X-ray source during the outburst. Irradiation prevents the disc from returning to the cool state until central accretion is greatly reduced. This happens only after most of the disc mass has been accreted by the central object, on a viscous time-scale, accounting naturally for the exponential decay of the outburst on a far longer time-scale (τ20–40 d) than seen in dwarf novae, without any need to manipulate the viscosity parameter α. The accretion of most of the disc mass in outburst explains the much longer recurrence time of SXTs compared with dwarf novae. This picture also suggests an explanation of the secondary maximum seen in SXT light curves about 50–75 d after the start of each outburst, since central irradiation triggers the thermal instability of the outer disc, adding to the central accretion rate one viscous time later. The X-ray outburst decay constant τ should on average increase with orbital period, but saturate at a roughly constant value ∼40 d for orbital periods longer than about a day. The bolometric light curve should show a linear rather than an exponential decay at late times (a few times τ). Outbursts of long-period systems should be entirely in the linear decay regime, as is observed in GRO J1744−28. UV and optical light curves should resemble the X-rays but have decay time-scales up to 2–4 times longer.  相似文献